[Fe/H] vs. ⟨R⟩ (top), ⟨R_peri⟩ (middle), and ⟨R_apo⟩ (bottom) for all stars in each MMR subgroup; their 2D-Gaussian kernel densities are also displayed along with those from the Solar group. The dotted, dashed, and dot-dashed black curves respectively depict the 3.3, 8, and 11 Gyr models described in Magrini et al. (2009). In all MMR subgroups, the values of [Fe/H] are very high even at large radii. Note that for each case (⟨R⟩, ⟨R_peri⟩, and ⟨R_apo⟩) the x-axis range is not the same to enable a better visualisation of the groups.